The Virgo detector contributed to the observations in the O3 observing run and increased its sensitivity from the initial 46 up to 60 Mpc during the run. The detector has undergone to a series of improvements since the end of the O3 observing run in view of O4, as the implementation of an additional recycling cavity at the output of the interferometer – the Signal Recycling cavity (SRC) – to broaden the sensitivity band, the Frequency Dependent Squeezing (FDS) to reduce quantum noise at all frequencies, and a new higher power laser. Some criticality have emerged mainly due to the presence in Virgo of marginally stable recycling cavities with respect to the stable recycling cavities present in the LIGO detectors, which increases the difficulty in controlling the interferometer in presence of defects as those introduced by the high power on the mirrors. This resulted in a delayed joining the O4 run due to a longer than expected commissioning phase. At present the detector is running with a lower laser power (and a lower sensitivity w.r.t. the project design). A new stop of about 2 yr is planned between O4 and O5 starting in 2027, to implement new upgrades (phase II). To improve the stability of the interferometer, we are considering a large upgrade to introduce stable cavities and this will imply heavy infrastructural works also with the minimal design. The aim is to reach a Binary Neutron Star (BNS) sensitivity larger than 100 Mpc. Plans are being made for the post-O5 period as a bridge between 2nd and 3rd generation detectors and a new collaborative effort has born under the name of Virgo nEXT with the aim to keep and push the infrastructure and maintain alive the community.
Sebastiano Aiello, Arnauld Albert, Sergio Alves Garre, Zineb Aly, Fabrizio Ameli, Michel Andre, Giorgos Androulakis, Marco Anghinolfi, Mancia Anguita, Gisela Anton, Miquel Ardid, Julien Aublin, Christos Bagatelas, Giancarlo Barbarino, Bruny Baret, Suzan Basegmez du Pree, Anastasios Belias, Meriem Bendahman, Edward Berbee, Ad van den Berg, Vincent Bertin, Vincent van Beveren, Simone Biagi, Andrea Biagioni, Matthias Bissinger, Markus Boettcher, Jihad Boumaaza, Mohammed Bouta, Mieke Bouwhuis, Cristiano Bozza, Horea Brânzas, Ronald Bruijn, Jurgen Brunner, Ernst-Jan Buis, Raffaele Buompane, Jose Busto, Barbara Caiffi, David Calvo, Antonio Capone, Victor Carretero, Paolo Castaldi, Silvia Celli, Mohamed Chabab, Nhan Chau, Andrew Chen, Silvio Cherubini, Vitaliano Chiarella, Tommaso Chiarusi, Marco Circella, Rosanna Cocimano, Joao A. Coelho, Alexis Coleiro, Marta Colomer Molla, Stephane Colonges, Rosa Coniglione, Imanol Corredoira, Paschal Coyle, Alexandre Creusot, Giacomo Cuttone, Antonio D'Amico, Antonio D’Onofrio, Richard Dallier, Mauro De Palma, Irene Di Palma, Antonio Díaz, Didac Diego-Tortosa, Carla Distefano, Alba Domi, Roberto Donà, Corinne Donzaud, Damien Dornic, Manuel Dörr, Doriane Drouhin, Thomas Eberl, Ahmed Eddyamoui, Thijs van Eeden, Daan van Eijk, Imad El Bojaddaini, Dominik Elsaesser, Alexander Enzenhoefer, Victor Espinosa Rosell, Paolo Fermani, Giovanna Ferrara, Miroslav Filipovic, Francesco Filippini, Luigi Antonio Fusco, Omar Gabella, Tamas Gal, Alfonso Andres Garcia Soto, Fabio Garufi, Yoann Gatelet, Nicole Geißelbrecht, Lucio Gialanella, Emidio Giorgio, Sara Gozzini, Rodrigo Gracia, Kay Graf, Dario Grasso, Giuseppe Grella, Daniel Guderian, Carlo Guidi, Steffen Hallmann, Hassane Hamdaoui, Hans van Haren, Aart Heijboer, Amar Hekalo, Juan Hernández-Rey, Jannik Hofestädt, Feifei Huang, Walid Idrissi Ibnsalih, Alin Ilioni, Giulia Illuminati, Clancy James, Peter Jansweijer, Maarten de Jong, Paul de Jong, Bouke Jisse Jung, Matthias Kadler, Piotr Kalaczyński, Oleg Kalekin, Uli Katz, Nafis Khan Chowdhury, Giorgi Kistauri, Frits van der Knaap, Els Koffeman, Paul Kooijman, Antoine Kouchner, Michael Kreter, Vladimir Kulikovskiy, Robert Lahmann, Giuseppina Larosa, Remy Le Breton, Ornella Leonardi, Francesco Leone, Emanuele Leonora, Jean Lesrel, Giuseppe Levi, Massimiliano Lincetto, Miles Lindsey Clark, Thomas Lipreau, Alessandro Lonardo, Fabio Longhitano, Daniel Lopez-Coto, Lukas Maderer, Jerzy Mańczak, Karl Mannheim, Annarita Margiotta, Antonio Marinelli, Christos Markou, Lilian Martin, Juan Martínez-Mora, Agnese Martini, Fabio Marzaioli, Stefano Mastroianni, Safaa Mazzou, Karel Melis, Gennaro Miele, Pasquale Migliozzi, Emilio Migneco, Piotr Mijakowski, Luis Miranda Palacios, Carlos Mollo, Mauro Morganti, Michael Moser, Abdelilah Moussa, Rasa Muller, David Muñoz Pérez, Paolo Musico, Mario Musumeci, Lodewijk Nauta, Sergio Navas, Carlo Nicolau, Brian Fearraigh, Mitchell O’Sullivan, Mukharbek Organokov, Angelo Orlando, Juan Palacios González, Gogita Papalashvili, Riccardo Papaleo, Cosimo Pastore, Alice Păun, Gabriela Păvălaş, Giuliano Pellegrini, Carmelo Pellegrino, Mathieu Perrin-Terrin, Paolo Piattelli, Camiel Pieterse, Konstantinos Pikounis, Ofelia Pisanti, Chiara Poirè, Vlad Popa, Thierry Pradier, Gerd Pühlhofer, Sara Pulvirenti, Omphile Rabyang, Fabrizio Raffaelli, Nunzio Randazzo, Soebur Razzaque, Diego Real, Stefan Reck, Giorgio Riccobene, Marc Richer, Stephane Rivoire, Alberto Rovelli, Francisco Salesa Greus, Dorothea F. Samtleben, Agustin Sánchez Losa, Matteo Sanguineti, Andrea Santangelo, Domenico Santonocito, Piera Sapienza, Jan-Willem Schmelling, Jutta Schnabel, Johannes Schumann, Jordan Seneca, Irene Sgura, Rezo Shanidze, Ankur Sharma, Francesco Simeone, Anna Sinopoulou, Bernardino Spisso, Maurizio Spurio, Dimitris Stavropoulos, Jos Steijger, Simona Stellacci, Mauro Taiuti, Yahya Tayalati, Enrique Tenllado, Tarak Thakore, Steven Tingay, Ekaterini Tzamariudaki, Dimitrios Tzanetatos, Veronique Van Elewyck, George Vasileiadis, Federico Versari, Salvo Viola, Daniele Vivolo, Gwenhael de Wasseige, Jörn Wilms, Rafał Wojaczyński, Els de Wolf, Dmitry Zaborov, Sandra Zavatarelli, Angela Zegarelli, Daniele Zito, Juan de Dios Zornoza, Juan Zúñiga, Natalia Zywucka
The KM3NeT infrastructure consists of two deep-sea neutrino telescopes being deployed in the Mediterranean Sea. The telescopes will detect extraterrestrial and atmospheric neutrinos by means of the incident photons induced by the passage of relativistic charged particles through the seawater as a consequence of a neutrino interaction. The telescopes are configured in a three-dimensional grid of digital optical modules, each hosting 31 photomultipliers. The photomultiplier signals produced by the incident Cherenkov photons are converted into digital information consisting of the integrated pulse duration and the time at which it surpasses a chosen threshold. The digitization is done by means of time to digital converters (TDCs) embedded in the field programmable gate array of the central logic board. Subsequently, a state machine formats the acquired data for its transmission to shore. We present the architecture and performance of the front-end firmware consisting of the TDCs and the state machine.
With the observation of the gravitational wave event of August 17th 2017 the multi-messenger astronomy era has definitely begun. With the opening of this new panorama, it is necessary to have new instruments and a perfect coordination of the existing observatories. Crystal Eye is a detector aimed at the exploration of the electromagnetic counterpart of the gravitational waves. Such events generated by neutron stars’ mergers are associated with gamma-ray bursts (GRB). At present, there are few instruments in orbit able to detect photons in the energy range going from tens of keV to few MeV. These instruments belong to two different old observation concepts: the all sky monitors (ASM) and the telescopes. The detector we propose is a crossover technology, the Crystal Eye: a wide field of view observatory in the energy range from 10 keV to 10 MeV with a pixelated structure. A pathfinder will be launched with Space RIDER in 2022. We here present the preliminary results of the characterization of the first pixel.
Annarita Margiotta, Antonio Marinelli, Christos Markou, Gregory Martignac, Lilian Martin, Juan Martínez-Mora, Agnese Martini, Fabio Marzaioli, Safaa Mazzou, Rosa Mele, Karel Melis, Pasquale Migliozzi, Emilio Migneco, Piotr Mijakowski, Luis Miranda, Carlos Mollo, Mauro Morganti, Michael Moser, Abdelilah Moussa, Rasa Muller, Paolo Musico, Mario Musumeci, Lodewijk Nauta, Sergio Navas, Carlo Nicolau, Christine Nielsen, Brian Fearraigh, Mukharbek Organokov, Angelo Orlando, Gogita Papalashvili, Riccardo Papaleo, Cosimo Pastore, Gabriela Păvălaş, Giuliano Pellegrini, Carmelo Pellegrino, Mathieu Perrin-Terrin, Paolo Piattelli, Camiel Pieterse, Konstantinos Pikounis, Ofelia Pisanti, Chiara Poirè, Georgia Polydefki, Vlad Popa, Maarten Post, Thierry Pradier, Gerd Pühlhofer, Sara Pulvirenti, Liam Quinn, Fabrizio Raffaelli, Nunzio Randazzo, Antonio Rapicavoli, Soebur Razzaque, Diego Real, Stefan Reck, Jonas Reubelt, Giorgio Riccobene, Marc Richer, Louis Rigalleau, Alberto Rovelli, Ilenia Salvadori, Dorothea F. Samtleben, Agustin Sánchez Losa, Matteo Sanguineti, Andrea Santangelo, Domenico Santonocito, Piera Sapienza, Jan-Willem Schmelling, Jutta Schnabel, Virginia Sciacca, Jordan Seneca, Irene Sgura, Rezo Shanidze, Ankur Sharma, Francesco Simeone, Anna Sinopoulou, Bernardino Spisso, Maurizio Spurio, Dimitris Stavropoulos, Jos Steijger, Simona Stellacci, Bruno Strandberg, Dominik Stransky, Mauro Taiuti, Yahya Tayalati, Enrique Tenllado, Tarak Thakore, Paul Timmer, Steven Tingay, Ekaterini Tzamarias, Dimitrios Tzanetatos, Veronique Van Elewyck, Federico Versari, Salvo Viola, Daniele Vivolo, Gwenhael de Wasseige, Jörn Wilms, Rafał Wojaczyński, Els de Wolf, Dmitry Zaborov, Angela Zegarelli, Juan Zornoza, Juan Zúñiga, Vasilis Panagopoulos, Sebastiano Aiello, Fabrizio Ameli, Michel Andre, Giorgos Androulakis, Marco Anghinolfi, Gisela Anton, Miquel Ardid, Julien Aublin, Christos Bagatelas, Giancarlo Barbarino, Bruny Baret, Suzan Basegmez du Pree, Anastasios Belias, Meriem Bendahman, Edward Berbee, Ad van den Berg, Vincent Bertin, Vincent van Beveren, Simone Biagi, Andrea Biagioni, Matthias Bissinger, Pascal Bos, Jihad Boumaaza, Simon Bourret, Mohammed Bouta, Gilles Bouvet, Mieke Bouwhuis, Cristiano Bozza, Horea Brânzaş, Max Briel, Marc Bruchner, Ronald Bruijn, Jurgen Brunner, Ernst-Jan Buis, Raffaele Buompane, Jose Busto, David Calvo, Antonio Capone, Silvia Celli, Mohamed Chabab, Nhan Chau, Silvio Cherubini, Vitaliano Chiarella, Tommaso Chiarusi, Marco Circella, Rosanna Cocimano, Joao A. Coelho, Alexis Coleiro, Marta C. Molla, Stephane Colonges, Rosa Coniglione, Paschal Coyle, Alexandre Creusot, Giacomo Cuttone, Antonio D’Amico, Antonio D’Onofrio, Richard Dallier, Mauro De Palma, Irene Di Palma, Antonio Díaz, Didac Diego-Tortosa, Carla Distefano, Alba Domi, Roberto Donà, Corinne Donzaud, Damien Dornic, Manuel Dörr, Mora Durocher, Thomas Eberl, Thijs van Eeden, Imad El Bojaddaini, Hassnae Eljarrari, Dominik Elsaesser, Alexander Enzenhöfer, Paolo Fermani, Giovanna Ferrara, Miroslav Filipovic, Luigi A. Fusco, Deepak Gajanana, Tamas Gal, Alfonso Garcia Soto, Fabio Garufi, Lucio Gialanella, Emidio Giorgio, Sara Gozzini, Rodrigo Gracia, Kay Graf, Dario Grasso, Timothee Grégoire, Giuseppe Grella, Daniel Guderian, Carlo Guidi, Steffen Hallmann, Hassane Hamdaoui, Hans van Haren, Aart Heijboer, Amar Hekalo, Universitat de València Hernández-Rey, Jannik Hofestädt, Feifei Huang, Enrique Santiago, Giulia Illuminati, Clancy James, Peter Jansweijer, Martijn Jongen, Maartin de Jong, Paul de Jong, Matthias Kadler, Piotr Kalaczyński, Oleg Kalekin, Uli Katz, Nafis Khan Chowdhury, Frits van der Knaap, Els N. Koffeman, Paul Kooijman, Antoine Kouchner, Michael Kreter, Vladimir Kulikovskiy, Robert Lahmann, Giuseppina Larosa, Remy Le Breton, Francesco Leone, Emanuele Leonora, Giuseppe Levi, Massimiliano Lincetto, Miles Lindsey Clark, Alessandro Lonardo, Fabio Longhitano, Daniel Lopez-Coto, Giuliano Maggi, Jerzy Mańczak, Karl Mannheim
The KM3NeT research infrastructure being built at the bottom of the Mediterranean Sea will host water-Cherenkov telescopes for the detection of cosmic neutrinos. The neutrino telescopes will consist of large volume three-dimensional grids of optical modules to detect the Cherenkov light from charged particles produced by neutrino-induced interactions. Each optical module houses 31 3-in. photomultiplier tubes, instrumentation for calibration of the photomultiplier signal and positioning of the optical module, and all associated electronics boards. By design, the total electrical power consumption of an optical module has been capped at seven Watts. We present an overview of the front-end and readout electronics system inside the optical module, which has been designed for a 1-ns synchronization between the clocks of all optical modules in the grid during a life time of at least 20 years.
With the observation of the gravitational wave event of August 17th 2017 and then with those of the extragalactic neutrino of September 22nd, the multi messenger astronomy era has definitely begun. With the opening of this new panorama, it is necessary to have a perfect coordination of the several observatories. Crystal Eye is an experiment aimed at the exploration of the electromagnetic counterpart of the gravitational wave events, that represent the missing observational link between short Υ-ray bursts and gravitational waves from neutron star mergers. The experiment we propose is a wide field of view observatory. The Crystal Eye objectives will be: to alert the community about events containing soft X-ray and low energy Υ-ray, to monitor long-term variabilities of X-ray sources, to stimulate multi-wavelength observations of variable objects, and to observe diffuse cosmic soft X-ray emissions.
KEYWORDS: Control systems, Prototyping, Data acquisition, Sensors, Interferometry, Environmental monitoring, Control systems design, Mirrors, Computing systems, Digital signal processing
In this paper we describe the architecture and the performances of a hybrid modular acquisition and control
system prototype for environmental monitoring and geophysics. The system, an alternative to a VME-UDP/IP
based system, is based on a dual-channel 18-bit low noise ADC and a 16-bit DAC module at 1 MHz. The
module can be configured as stand-alone or mounted on a motherboard as mezzanine. Both the modules and
the motherboard can send/receive the configuration and the acquired/correction data for control through a
standard EPP parallel port to a standard PC for the real-time computation. The tests have demonstrated that a
distributed control systems based on this architecture exhibits a delay time of less than 25 us on a single channel,
i.e a sustained sampling frequency of more than 40 kHz (and up to 80 kHz). The system is now under extensive
test in the remote controls of seismic sensors (to simulate a geophysics networks of sensors) of a large baseline
suspended Michelson interferometer.
KEYWORDS: Control systems, Prototyping, Data acquisition, Sensors, Interferometry, Control systems design, Mirrors, Environmental monitoring, Computing systems, Digital signal processing
In this paper we describe the architecture and the performances of a hybrid modular acquisition and control
system prototype for environmental monitoring and geophysics. The system, an alternative to a VME-UDP/IP
based system, is based on a dual-channel 18-bit low noise ADC and a 16-bit DAC module at 1 MHz. The
module can be configured as stand-alone or mounted on a motherboard as mezzanine. Both the modules and
the motherboard can send/receive the configuration and the acquired/correction data for control through a
standard EPP parallel port to a standard PC for the real-time computation. The tests have demonstrated that a
distributed control systems based on this architecture exhibits a delay time of less than 25 us on a single channel,
i.e a sustained sampling frequency of more than 40 kHz (and up to 80 kHz). The system is now under extensive
test in the remote controls of seismic sensors (to simulate a geophysics networks of sensors) of a large baseline
suspended Michelson interferometer.
In this paper we describe the architecture and the performances of a hybrid modular acquisition and control
system prototype for environmental monitoring and geophysics. The system, an improvement of a VME-UDP/IP
based system we developed for interferometric detectors of gravitational waves, is based on a dual-channel 18-bit low noise ADC, a 16-bit DAC module at 1MHz, and a 20-bit slower ADC necessary for the acquisition
of an external calibration signal. The module can be configured as stand-alone or mounted on a motherboard
as mezzanine in parallel with other modules. Both the modules and the motherboard can send/receive the
configuration and the acquired/correction data for control through a standard EPP parallel port to a standard
PC, where the real-time computation is performed. Experimental tests have demonstrated that the distributed
control systems implemented with this architecture exihibit a delay time of less than 25 μs on a single channel, that
is a sustained sampling frequency of more than 40kHz. The system is now under extensive test in two different
experiments: the remote control and data acquisition of a set of seismometers, velocimeters and accelerometers
to simulate a geophysics networks of sensors and the remote control of the end mirrors of a suspended Michelson
interferometer through electrostatic actuators for interferometric detectors of gravitational waves.
Laser interferometry is one of the most sensitive methods for small displacement measurement for scientific and
industrial applications, whose wide diffusion in very different fields is due not only to the high sensitivity and
reliability of laser interferometric techniques, but also to the availability of not expensive optical components
and high quality low-cost laser sources. Interferometric techniques have been already successfully applied also to
the design and implementation of very sensitive sensors for geophysical applications. In this paper we describe
the architecture and the expected theoretical performances of a laser interferometric velocimeter for seismic
waves measurement. We analyze and discuss the experimental performances of the interferometric system,
comparing the experimental results with the theoretical predictions and with the performances of a state-of the
art commercial accelerometer. The results obtained are very encouraging, so that we are upgrading the system
in order to measure the local acceleration of the mirrors and beam splitter of the velocimeter using an ad hoc
designed monolithic accelerometers for low frequency direct measurement of the seismic noise.
Laser interferometry is one of the most sensitive methods for small displacement measurement for scientific and
industrial applications, whose wide diffusion in very different fields is due not only to the high sensitivity and
reliability of laser interferometric techniques, but also to the availability of not expensive optical components
and high quality low-cost laser sources. Interferometric techniques have been already successfully applied also to
the design and implementation of very sensitive sensors for geophysical applications. In this paper we describe
the architecture and the expected theoretical performances of a laser interferometric velocimeter for seismic
waves measurement. We analyze and discuss the experimental performances of the interferometric system,
comparing the experimental results with the theoretical predictions and with the performances of a state-of-the
art commercial accelerometer. The results obtained are very encouraging, although few problems, mainly related
to the sensitivity and stability of the interferometric system, have to be better studied.
In this paper we describe the architecture and the performances of a hybrid modular acquisition and control
system prototype we developed in Napoli for the implementation of geographycally distributed monitoring and
control systems. The system, an improvement of a VME-UDP/IP based system developed by our group for
interferometric detectors of gravitational waves, is based on a dual-channel 18-bit low noise ADC and 16-bit DAC
module at 1 MHz, managed by an ALTERA FPGA, that can be used standalone or mounted as mezzanine (also
in parallel with other modules) on a motherboard. Both the modules and the motherboard can send/receive
the configuration and the acquired/correction data for control through a standard EPP parallel port to an
external PC, where the real-time computation is performed. Experimental tests have demonstrated that this
architeture allows the implementation of distributed control systems, using a standard laptop PC for the realtime
computation, with delay time &Dgr;t < 30 &mgr;s on a single channel, that is a sustained sampling frequency
fc > 30kHz. Each module is also equipped with a 20-bit slower ADC necessary for the acquisition of an
external calibration signal. The system is now under extensive test in two different experiments, i.e. the control
of a Michelson Interferometer to be used as Velocimeter for Seismic Waves in Geophysics and the control of the
end mirrors a suspended Michelson Interferometer through electrostatic actuators, a prototype for mirror control
for Interferometric Detectors of Gravitational Waves.
This papers describes a new low-frequency seismic sensor for geophysical applications. The instrument is basically
a monolithic tunable folded pendulum with an interferometric readout system, that can be configured as
seismometer or as accelerometer. The monolithic mechanical design and the introduction of a laser interferometric
technique for the readout implementation make it a very sensitive and compact instrument with a very good
immunity to environmental noises. Preliminary tests on the mechanical performances of the monolithic structure
and on the optical reaodut have been performed. Interesting result is the measured resonant frequency of the
instrument of ≈ 150mHz obtained with a rough tuning, demonstrating the feasibility of a resonant frequency
of the order of 5mHz with a more refined tuning. The mechanics of the seismic sensor, the optical scheme of
the readout system, the theoretical predictions and the preliminary experimental performances as seismometer
are discussed in detail, together with the foreseen further improvements.
KEYWORDS: Control systems, Remote sensing, Prototyping, Data acquisition, Sensing systems, Environmental monitoring, Data fusion, Sensors, Computing systems, Digital signal processing
In this paper we describe the architecture and the performances of a hybrid acquisition system prototype we implemented in Napoli for remote sensing applications, which allow the fusion of multi-source data produced by environmental noise sources. In particular, we discuss how the system is able to integrate geographically distributed sensors for seismic, electromagnetic, acoustic, etc. noises, sampled at different frequencies, too. This system is an improvement of the environmental monitoring system developed by our group for interferometers for gravitational wave detection. In this paper we discuss the system, together with its characteristics and performances in connection with its application for the implementation of a geographically distributed monitoring system.
Giuseppe Martellotti, P. Annis, J. Brunner, S. Buontempo, Maarten de Jong, D. Depedis, A. Ereditato, Jean-Paul Fabre, D. Frekers, Annette Frenkel, F. Galeazzi, F. Garufi, Sergei Golovkin, Alexandre Gorin, G. Gregoire, M. Gruwe, K. Harrison, K. Hoepfner, Joop Konijn, Eugene Kozarenko, Igor Kreslo, Andrei Medvedkov, L. Michel, Chantal Mommaert, M. Mondardini, Jaap Panman, Gianni Penso, Yuri Petukhov, F. Riccardi, W. Siegmund, Richard Strack, Valeri Tyukov, Vladimir Vasil'chenko, P. Vilain, Gaston Wilquet, K. Winter, Henry Wong, Konstatin Zymin
We abstract developed a new technique that allows the trajectories of ionizing particles to be imaged with very high spatial and temporal resolution. This technique, developed for future experiments in high-energy physics, may also be applied in other field. Central to the technique is a detector consisting of a bundle of thin, glass capillaries filled with a liquid scintillator of high refractive index. These liquid-core scintillating fibers act simultaneously as a detector of charged particles and as an image guide. Track images seen at the readout end of the capillary bundle are amplified by an optoelectronic chain consisting of a set of image- intensifier tubes and read by a photosensitive CCD camera. We report here on results obtained with detector prototypes. A spatial resolution of 6-14 micrometers , dependent on image magnification prior to readout, has been obtained with 16 micrometers capillaries. The high scintillation efficiency of the liquid scintillator used and a large light attenuation length-- approximately 3 m for 20 micrometers capillaries--result in hit densities along the track of a minimum-ionizing particle of 8.5 mm-1 and 3.5 mm-1 at distances from the readout window of approximately 2 cm and approximately 1 m respectively. The radiation resistance of the detector is an order of magnitude greater than that of other types of tracking device of comparable performance. To complement the detector we have been developing a new readout system based around a gateable vacuum image pipeline (VIP) and an electron- bombarded CCD camera. These increase the spatial and temporal resolution obtained with detector and render it particlarly attractive as a microvertex detector for the observation of short-lived particles in high-energy physics experiments performed with evelated interaction rates.
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